Stochastic oscillations in A-type and related stars

Strong evidence, from different types of observations, suggests that convective motion is present in the very outer envelopes of A-type and early F-type stars. Theoretical models also predict that stars situated in the lower part of the classical instability strip should have shallow, but still effective, turbulent convective envelopes that can excite solar-like oscillations. In the more massive B-type stars, the convection in the very outer layers disappears, but there are still convective regions throughout the star which could excite pulsations stochastically. In this article I give an overview of recent observations, and discuss upper main-sequence pulsators such as delta Scuti, gamma Doradus and roAp stars in the context of solar-like oscillations.